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Among a number of active galactic nuclei (AGNs) that drive ionized outflowsin X-rays, a low-redshift (z = 0.184) quasar, PDS 456, is long known to exhibitone of the exemplary ultra-fast outflows (UFOs). However, the physical processof acceleration mechanism is yet to be definitively constrained. In this work,we model the variations of the Fe K UFO properties in PDS 456 over many epochsin X-ray observations in the context of magnetohydrodynamic (MHD)accretion-disk winds employed in our earlier studies of similar X-rayabsorbers. We applied the model to the 2013/2014 XMM-Newton/NuSTAR spectra todetermine the UFO's condition; namely, velocity, ionization parameter, columndensity and equivalent width (EW). Under some provisions on the dependence ofX-ray luminosity on the accretion rate applicable to near-Eddington state, ourphotoionization calculations, coupled to a 2.5-dimensional MHD-driven windmodel, can further reproduce the observed correlations of the UFO velocity andthe anti-correlation of its EW with X-ray strength of PDS 456. This workdemonstrates that UFOs, even without radiative pressure, can be driven as anextreme case purely by magnetic interaction while also producing the observedspectrum and correlations.

Variable Nature of Magnetically-Driven Ultra-Fast Outflows